Big Cluster Elliptical Galaxies Formed First

July 20, 2006

Cluster galaxies are older than field galaxies;and the age gap increases with mass...

NASA/ESA Image

Figure 1: The central 75 arcsecond x 45 arcsecond of the cluster RXJ1226.9+3332 at redshift 0.89. The image covers approximately 0.6 Mpc x 0.35 Mpc at the distance of the cluster. The early-type galaxies in the cluster appear yellow/orange. The many faint blue and very elongated objects are gravitationally lensed background galaxies. The image is made from HST/ACS observations in F606W (blue) and F814W (red).

Sperello di Serego Alighieri (Observatorio Astrofisico di Arcetri), Barbara Lanzoni (Observatorio Astronomico di Bologna) and Inger Jørgensen (Gemini Observatory) have just released new Gemini/HST results confirming that big galaxies form first and smaller ones later. This spread happens both in rich galaxy clusters and in the general low density field. Furthermore, they show that the first early-type galaxies that formed were the most massive ones in galaxy clusters.

As the 100th refereed paper based on GMOS-North data, this work represents a significant milestone for the productivity of the Gemini telescopes and its instrument set. GMOS-North was commissioned on the Gemini North Telescope in late 2001.

Figure 2: The lookback time to formation for the individual galaxies in the sample versus the galaxy masses. Field galaxies at redshifts z∼1 - black and blue points, cluster galaxies at redshifts 0.8-0.9 - red points.

There are now many studies of the distant universe that have explored the formation and evolution of galaxies when the universe was less than half its current age (see related Gemini stories from: January 5, 2004,May 18, 2004 and July 7, 2004). The emerging view is that a significant fraction of the most massive galaxies were already in place only a few billions years following the Big Bang, and that the less massive galaxies take more time to assemble. Big ones, first; little ones after, and more slowly. This way of forming and evolving galaxies is referred to as the downsizing scenario. A different scenario is the hierarchical model with big galaxies building up slowly with time as they assemble from the coalescence of smaller galaxies or proto-galaxies.

A less known effect is that of the environment. Do galaxies form differently in the dense environment of clusters compared to the general field?

Figure 3: Top - The average lookback time to formation for the field galaxies (hatched) and cluster galaxies (open). Bottom - the difference between the lookback time to formation for galaxies in the clusters and in the field.

Galaxy clusters provide much denser environments than the general field. In works published during the last year, comparing two large galaxy clusters at redshift z = 0.835 and 0.892 with the nearby Coma Cluster, Jørgensen et al. demonstrated that low-mass galaxies have later and more prolonged star formation than massive ones. Figure 1 shows a color image of the redshift 0.892 cluster based on the HST imaging.

A clear and important result is the lack of recently formed massive early-type galaxies either in the field or in the clusters. In particular all early type galaxies with mass M > 3 x 1011 Msun have a lookback time to formation larger than 10 billion years (or zformation > 2). More massive galaxies are older than lower mass galaxies in all environments. Cluster galaxies are older than field galaxies of the same mass, clearly indicating that the high-density environment of the cluster has an impact. Furthermore, and this is a completely new result, the age difference between cluster and field galaxies of a same given mass increase as mass increases. This is shown in Figure 2 as the lookback time to formation versus the galaxy masses for the individual galaxies in the sample. Figure 3 shows the average lookback time versus galaxy masses, and the average time difference between the cluster and field galaxies versus galaxy masses.

Thus, the first early-type galaxies that formed in the universe were the most massive ones in galaxy clusters. The last to form are the low mass (early-type) galaxies in the field, they are quite contemporaneous to the cluster galaxies.

For more details see the article: "The influence of mass and environment on the evolution of early-type galaxies," by Sperello di Serego Alighieri, Barbara Lanzoni & Inger Jørgensen, 2006, The Astrophysical Journal Letters, in press (available from astro-ph/0607231). For results on the high redshift clusters, see the article: "The Fundamental Plane for z=0.8-0.9 Cluster Galaxies," by Inger Jørgensen et al., 2006, The Astrophysical Journal Letters, 639, L9-L12

The Gemini Observatory is an international collaboration with two identical 8-meter telescopes. The Frederick C. Gillett Gemini Telescope is located on Maunakea, Hawai'i (Gemini North) and the other telescope on Cerro Pachón in central Chile (Gemini South); together the twin telescopes provide full coverage over both hemispheres of the sky. The telescopes incorporate technologies that allow large, relatively thin mirrors, under active control, to collect and focus both visible and infrared radiation from space.

The Gemini Observatory provides the astronomical communities in five partner countries with state-of-the-art astronomical facilities that allocate observing time in proportion to each country's contribution. In addition to financial support, each country also contributes significant scientific and technical resources. The national research agencies that form the Gemini partnership include: the US National Science Foundation (NSF), the Canadian National Research Council (NRC), the Argentinean Ministerio de Ciencia, Tecnología e Innovación Productiva, the Brazilian Ministério da Ciência, Tecnologia e Inovação and the Chilean Comisión Nacional de Investigación Científica y Tecnológica (CONICYT). The observatory is managed by the Association of Universities for Research in Astronomy, Inc. (AURA) under a cooperative agreement with the NSF. The NSF also serves as the executive agency for the international partnership.